nEoS: Neutron Star Equation of State from hadron physics alone. (arXiv:1901.05271v1 [gr-qc])

nEoS: Neutron Star Equation of State from hadron physics alone. (arXiv:1901.05271v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Oter_E/0/1/0/all/0/1">Eva Lope Oter</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Windisch_A/0/1/0/all/0/1">Andreas Windisch</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Llanes_Estrada_F/0/1/0/all/0/1">Felipe J. Llanes-Estrada</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Alford_M/0/1/0/all/0/1">Mark Alford</a>

We contribute a publicly available set of tables and code to provide
Equations of State (EoS) for matter at neutron star densities. Our EoSes are
constrained only by input from hadron physics and fundamental principles,
without feedback from neutron star observations, and so without relying on
General Relativity. They can therefore be used to test General Relativity
itself, as well as modified gravity theories, with neutron star observables,
without logical circularity. We have adapted state of the art results from NN
chiral potentials for the low–density limit, pQCD results for the
asymptotically high-density EoS, and use monotonicity and causality as the only
restrictions for intermediate densities, for the EoS sets to remain as
model-independent as is feasible today.

http://arxiv.org/icons/sfx.gif